Table 3
Summary of the samples and data used in this paper.
Sample | Number of galaxies used here | Relevant references | Optical spectra | H I masses | Metallicity indicator | min log M⋆ (M⊙) | max log M⋆ (M⊙) | Notes |
---|---|---|---|---|---|---|---|---|
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
H IX | 10 | Lutz et al. (2017, 2018) | Y | Y | PP04 O3N2, N2 | 9.8 | 10.6 | |
IC 4857 | 1 | As H IX | Y | Y | PP04 O3N2, N2 | 10.5 | Member of the original CONTROL sample | |
HIPASS | 1796 | Dénes et al. (2014); Barnes et al. (2001); Meyer et al. (2004); Doyle et al. (2005) | N | Y | – | 8.0 | 11.5 | Biased towards H I-rich objects, maximal redshift 0.04, parent sample for H IX galaxies |
SDSS MPA-JHU | 60021 | Abazajian et al. (2009); Salim et al. (2007) | Y | N | PP04 O3N2 | 8.0 | 11.5 | To provide a benchmark mass-metallicity relation |
GASS with longslit spectroscopy | 96 | Catinella et al. (2018); Moran et al. (2012) | Y | Y | PP04 O3N2 | 10.0 | 10.82 | Longslit spectra typically out to 1 Petrosian 90% radius, see text for sample selection |
CALIFA | 227 | Sánchez et al. (2014) | Y | N | PP04 O3N2 | 9.0 | 11.2 | IFU data, the metallicity gradient is typically measured between 0.5 and 2 effective radii |
Notes. Column (1): name of the sample. Column (2): number of galaxies used in this paper. Column (3): references to the papers in which the sample and/or data are described in more detail. Column (4): whether (Y) or not (N) optical spectra are available for this sample. Column (5): whether (Y) or not (N) measurements of the H I mass are available for this sample. Column(6): which metallicity indicator was used to estimate the gas-phase metallicity. PP04 refers to Pettini & Pagel (2004). Columns (7) and (8): minimum and maximum stellar mass limit of the sample, respectively. Column (9): further notes.
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